Extended gas in Seyfert 2 galaxies: implications for the nuclear source

Transcription

1 Mon. Not. R. Astron. Soc. 341, (2003) Extended gas in Seyfert 2 galaxies: implications for the nuclear source Henrique A. Fraquelli, 1 T. Storchi-Bergmann 1 and N. A. Levenson 2 1 Instituto de Física, UFRGS, Porto Alegre, RS, Brazil 2 Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA Accepted 2003 January 7. Received 2002 December 19; in original form 2001 August 20 1 INTRODUCTION Ionized gas in Seyfert galaxies is observed extending from tens of parsecs up to several kiloparsecs from the nucleus. A number of studies have been published showing the spatial distribution of this gas in narrow-band images (Mulchaey, Wilson & Tsvetanov 1996a), which is usually elongated and in some cases presents a clear coneshaped morphology (Storchi-Bergmann, Wilson & Baldwin 1992a; Wilson et al. 1993). The extended ionized gas is usually identified with the narrowline region (NLR) of active galactic nuclei (AGN). Unger et al. (1987) have proposed a new terminology, extended narrow-line region (ENLR), to identify the outer parts of the extended ionized gas. The classical NLR would be the inner part, which shows kinematic signatures of interaction with a radio-emitting plasma or an accretion disc wind, usually indicating the presence of outflows (e.g. Crenshaw et al. 2000). Detailed studies of the NLR, available for a few Seyfert galaxies (e.g. Crenshaw et al. 2000; Crenshaw & Kraemer 2000; Ruiz et al. 2001) indicate typical extents of up to 300 pc from the nucleus. The ENLR would correspond to the ionized gas beyond the NLR, where the gas velocities seem to be con- ico@if.ufrgs.br ABSTRACT We use long-slit spectroscopic optical data to derive the properties of the extended emitting gas and the nuclear luminosity of a sample of 18 Seyfert 2 galaxies. From the emissionline luminosities and ratios we derive the density, reddening and mass of the ionized gas as a function of distance up to 2 4 kpc from the nucleus. Taking into account the geometric dilution of the nuclear radiation, we derive the radial distribution of covering factors and the minimum rate of ionizing photons emitted by the nuclear source. This number is an order of magnitude larger than that obtained from the rate of ionizing photons intercepted by the gas and measured from the Hα luminosity. A calibration is proposed to recover this number from the observed luminosity. The He II λ4686/hβ line ratio was used to calculate the slope of the ionizing spectral energy distribution (SED), which in combination with the number of ionizing photons allows the calculation of the hard -ray luminosities. These luminosities are consistent with those derived from -ray spectra in the eight cases for which such data are available and recover the intrinsic -ray emission in Compton-thick cases. Our method can thus provide reliable estimates of the -ray fluxes in Seyfert 2 galaxies for the cases where it is not readily available. We also use the ionizing SED and luminosity to predict the infrared luminosity under the assumption that it is dominated by reprocessed radiation from a dusty torus, and find a good agreement with the observed AS luminosities. Key words: galaxies: active galaxies: ISM galaxies: Seyfert -rays: galaxies. sistent with rotation within the galaxy (Peterson 1997). The ENLR emission could thus be attributed to interstellar gas at kiloparsec scales in the host galaxies ionized by the AGN nucleus, and photoionization by the nuclear source seems to be the main mechanism producing the observed emission (Morse, Raymond & Wilson 1996; Evans et al. 1999). This conclusion is supported by self-consistent models applied to the ENLR (e.g. Nazarova, O Brien & Ward 1997; Fraquelli, Storchi-Bergmann & Binette 2000, hereafter FSBB). Once we know which are the dominant physical processes at play in the ENLR, the extended ionized gas can provide a periscopic view of the nuclear region in Seyfert 2 galaxies, in which the ionizing source is hidden from direct view. By measuring the emissionline fluxes and ratios, and under the assumption that the emission lines are mainly produced by photoionization, gas properties such as mass, density and reddening, can be readily obtained, and the luminosities and spectral energy distribution (SED) of the ionizing sources. Most recent works on the ENLR of Seyfert galaxies are detailed studies of only one galaxy. In this paper, our goal is to analyse the data of a larger sample 18 Seyfert 2 galaxies, in order to look for common properties of the ionized gas and nuclear sources in Seyfert 2 galaxies. We have thus collected optical emission-line fluxes from long-slit data of the above sample at a typical spatial C 2003 RAS

2 450 H. A. Fraquelli, T. Storchi-Bergmann and N. A. Levenson sampling at the galaxy of pc. In this paper particular emphasis is placed on the derivation of the SED and luminosity of the central source, derived using the spatial distribution of emission-line fluxes and ratios along the ENLR. 2 OBSERVATIONS AND THE SAMPLE High signal-to-noise ratio long-slit spectra of 18 Seyfert 2 galaxies with extended high excitation emission were obtained using the Cassegrain Spectrograph at the Blanco 4-m telescope of the Cerro Tololo Inter-American Observatory (CTIO) on 1992 May, 1994 January and December. The seeing was 1 arcsec, the spectral resolution 6 Å and the spectral range of the observations was Å. The slit width corresponded to 2 arcsec on the sky. The slit was oriented along the maximum extent of the high excitation gas observed in narrow-band images centred on [O III] λ7 (Mulchaey et al. 1996a). The average scale is 240 pc arcsec 1, ranging from 48 pc arcsec 1 (for NGC 1386) to 570 pc arcsec 1 (for CGCG ). More detailed information concerning the longslit spectroscopy can be found in Cid Fernandes, Storchi-Bergmann & Schmitt (1998), where measurements of the absorption-line features as a function of distance from the nucleus are presented. The sample comprises approximately 40 per cent of the Seyfert 2 galaxies from the catalogue of Veron-Cetty & Veron (2000) with z < 0.02 and luminosity in the [O III] λ7 emission line larger than erg s 1, which could be observed from the southern hemisphere. In addition, it contains the galaxies CGCG and MCG , which obey the [O III] luminosity criterion but are somewhat more distant, with z = and 0.024, respectively. Six of these galaxies have ENLR images obtained using narrow-band filters published by Mulchaey et al. (1996a). Relevant information on the sample and observations are presented in Table 1: Hubble types (NED), radial velocity (RC3), absolute magnitude, date of the observations, position angle of the slit, scale, inclination of the galaxy (LEDA) and foreground Milky Way reddening. In the first column we include a number that was used to identify the galaxies in figures in the next sections. An asterisk identifies the galaxies with ENLR images in Mulchaey et al. (1996a). Table 1. Sample properties. 3 RESULTS Spectra were extracted using a 2-arcsec window centred on the optical nucleus. Off-nucleus spectra were also extracted using 2-arcsec windows up to approximately 10 arcsec from the nucleus, and ranging, on average, from 3 to 6 arcsec further out. The windows sizes can be recovered from Figs 2 4 (below) using the scales given in Table 1, considering that there are no gaps between windows. As the nuclear extractions include gas emission within a few hundred parsecs from the nucleus for our sample, it is dominated by the high surface brightness NLR emission. According to Unger et al. (1987) the edge between the NLR and the ENLR is defined by a change in the kinematic properties of the gas such that in the ENLR the FWHM drops below 45 km s 1 and the velocity field is characteristic of normal galactic rotation. Our spectral resolution does not allow the derivation of the kinematic properties of the ionized gas, precluding a clear separation between the NLR and ENLR. Nevertheless, recent works (e.g. Crenshaw et al. 2000; Ruiz et al. 2001) suggest an extent for the NLR of 300 pc. Thus, for our sample, the NLR should be mostly contained in the nuclear extraction with the exception of the closest galaxies NGC 1386, 5643 and 6300 (Table 1), for which the NLR could extend to the next one or two windows if the NLR size above can be considered characteristic of most Seyfert galaxies. Besides these caveats we decided to refer to the nuclear extraction as the NLR and the offnucleus ones as the ENLR, considering that these definitions do not change the main results of the present work. Sample spectra of both the nuclear and extranuclear regions are shown in Fig. 1. Line emission was detected up to 2 4 kpc from the nuclei. The fluxes of the emission lines were measured as a function of distance from the nuclei by fitting Gaussians to the line profiles. Uncertainties in the fluxes were mostly caused by uncertainties in the placement of the continuum and were thus estimated as the product of the full-width at half-maximum of the line (FWHM) by the root-mean square deviation of the local continuum fluxes. The angular distances were transformed to linear distances at the galaxies and corrected for inclination using the information listed in Table 1. Line luminosities were calculated adopting H 0 = 75 km s 1 Mpc 1. Id Galaxy Morph. v Distance M B Date PA Scale i E(B V ) G (km s 1 ) (Mpc) (mag) (deg) (pc arcsec 1 ) (deg) (mag) 1 ESO 417-G6 (R)SA0/a /7 Jan Fairall 316 S /7 Jan CGCG Sa /7 Jan IC 1816 (R L)SA:(s:)a /7 Jan AS S /6 Jan MCG SB(r)a /7 Jan Mrk 1210 Sa /6 Jan Mrk 607 Sa:sp /7 Jan NGC 1358 SAB(r)0/a /7 Jan NGC 1386 SB(s) /7 Jan NGC 3081 SAB(r)0/a /29 May NGC 5135 SB(1)ab /30 May NGC 5643 SAB(rs)c /29 May NGC 6300 SB(rs)b /29 May NGC 6890 SB(r)ab /30 May NGC 7130 Sa pec /30 May NGC 7582 SB(s)ab /7 Jan Mrk 348 SA(s)0/a /7 Dec

3 Extended gas in Seyfert 2 galaxies Reddening distributions We have used the Balmer decrement Hα/Hβ to derive the distribution of reddening as a function of distance from the nucleus in 14 of the sample galaxies. We corrected for foreground Milky Way extinction and assumed the intrinsic ratio of Hα/Hβ = 3.1 (Osterbrock 1989). The resulting E(B V ) ranges from 0.3 to along the ENLR, with typical nuclear values of E(B V ), as shown in Fig. 2. In the cases where we could not measure the Hβ emission line, because it was superposed on the Hβ absorption line from the stellar component, we interpolated the reddening determined for the neighbouring locations. Although this interpolation is uncertain we believe it is a better representation of the actual E(B V ) than using no reddening at all. For NGC 6300, AS and Fairall 316, Hβ is too weak to be measured in most locations. For these cases we have obtained only lower limits for E(B V ), which have been used to correct the emission-line fluxes. In eight galaxies we deduced lower reddening in the nuclear region compared with the neighbouring locations further out. This is contrary to what might be expected, considering the dusty environment of Seyfert 2 nuclei (Antonucci 1993; Martini & Pogge 1999). Figure 1. Sample of some spectra used in this work. This type of variation of E(B V ) with radial distance had been previously found by Veilleux et al. (1995) for one Seyfert 2 galaxy and two LINERs out of a sample of 19 AGNs. They considered two possibilities. The first is that some Seyfert galaxies have a smaller amount of dust in the nucleus owing to dust destruction/expulsion by the ionizing radiation field generated in the AGN and/or by shocks. The second possibility is complex optical depth effects such that the inner regions could be optically thick to the optical emission. We attribute the higher incidence of this kind of behaviour in our work as compared with that of Veilleux et al. (1995) to the better spatial resolution of our data, as the data-taking procedure of Veilleux et al. was not optimized to obtain spatial information on the objects of their sample. In order to investigate whether the reddening behaviour could be a result of the fact that we did not take into account the underlying absorption owing to the contribution of the stellar population (which can be large in the case of Hβ) we have attempted to correct our data for this effect. First, we adopted a constant value of 2 Å for the equivalent width of both Hβ and Hα absorptions, a procedure frequently used in previous works. The result was many negative values for E(B V ), indicating that Hβ was overestimated. We have then used the spectrum of the nucleus of the normal galaxy

4 452 H. A. Fraquelli, T. Storchi-Bergmann and N. A. Levenson Figure 2. NGC 6684 to correct the spectra for the underlying absorption. This method did not give negative values for E(B V ) and made the distribution flatter only for two of the eight galaxies for which we had found smaller E(B V ) values at the nucleus. We thus conclude that the effect is real. The reddening was used to correct all emission-line fluxes, adopting the Seaton (1979) reddening law. 3.2 Electron density distributions The electron density distribution, derived from the emission-line ratio [S II] λ6731/[s II] λ6717 (Osterbrock 1989) is shown in Fig. 3 for 14 galaxies of our sample. For CGCG the [S II] emission lines could not to be measured. The gas at the nucleus has densities in the range 300 n e cm 3, which decrease outwards down to the low-density limit, assumed to be 50 cm 3, at the most distant locations (>2 kpc) from the nucleus. The nuclear regions have an average density of 440 ± 200 cm 3, similar to that obtained by Veilleux et al. (1995; 430 cm 3 ). 3.3 Luminosity distributions We have calculated the luminosities in the emission lines [O III] and Hα as well as in the continuum underlying [O III] along the r (parsec) E(B V ) as a function of the distance from the nucleus for 15 Seyfert 2 galaxies. ENLR from the emission-line fluxes and distances listed in Table 1. In order to allow a comparison among all galaxies of the sample, we have divided the integrated luminosity in each window by the corresponding area in square parsecs at the galaxy. These surface luminosity distributions L area corrected for the galactic and internal reddening, obtained in Section 3.1 are shown in Fig. 4. The [O III] surface luminosity distributions are, on average, more centrally peaked than those of [O II] λ3727 and Hα. This means that the excitation is higher close to the nucleus, with the ionization parameter seen by the gas decreasing with radius. The possible presence of H II regions in the disc of the host galaxies will also contribute to this behaviour. Fig. 5 shows a comparison between the nuclear surface luminosities in [O III] and Hα, showing that most of the galaxies of our sample present a nuclear ratio [O III]/Hα roughly constant with luminosity, with a ratio of approximately 3 4. We fitted a power-law function F = F 0 r δ to the surface luminosity distributions above, and to the density of the ionized gas obtained from the [S II] ratio. The fitting parameters are shown in Table 2 where L 0 corresponds to the surface luminosities at 100 pc from the nucleus. The [O III] luminosity falls faster with the radius than the Hα luminosity, with an average index for the power law of δ = 3.2 ± 0.8, excluding from the average the galaxies with poor fits

5 Extended gas in Seyfert 2 galaxies r (parsec) Figure 3. Electron density obtained from [S II] ratio as a function of the distance from the nucleus. Open symbols are locations where n e is the in low-density limit (assumed 50 cm 3 ). (identified by colons in the fitting parameters) due in most cases to an insufficient number of data points. For the Hα luminosity the average index is 2.4 ± 0.7. The gas density has an average index of δ = 0.9 ± 0.3. In order to assess the meaning of the above distributions, we use Osterbrock (1989) to express the Hβ luminosity of a nebula with a filling factor ɛ and ionized gas density n (assuming that n e = n ions = n) as L Hβ = α eff Hβ hν Hβ n 2 ɛ dv, (1) where dv is the element of volume and α eff Hβ is the effective Hβ recombination coefficient. In the locations where L Hβ could not be measured its value was obtained from the corrected Hα luminosity. If we assume that ɛ and n are constant within each window, we obtain L Hβ = α eff Hβ hν Hβ n 2 ɛv tot = α eff Hβ hν Hβn 2 V gas, (2) where V tot is the total volume corresponding to each window, and V gas = ɛv tot is the effective volume occupied by the ionized gas. Using the average indices for L Hα and n distributions we obtain, from equation (2) above, V gas r. However, considering the uncertainties, this result is also consistent with V gas constant along the ENLR. 3.4 Surface mass distribution of the ionized gas The ionized gas mass (integrated in the extraction windows) was obtained from the Hβ luminosity and the gas density (Peterson 1997) using the expression below: M H + = L41 Hβ n e M, (3) where L 41 Hβ is the Hβ luminosity in units of 1041 erg s 1, n e is the electron density in units of cm 3 and M H + is the ionized gas mass (in solar units) within the extracted window. We point out that M H + is a lower limit for the windows where the density is lower than the adopted 50 cm 3 (open symbols in Fig. 3). The total ionized gas and the nuclear (NLR) gas masses are listed in Table 3. The total mass, including the contributions of nucleus (NLR) and ENLR range from 10 5 to 10 7 M Inspecting the narrow-band images of the galaxies of our sample available in Mulchaey et al. (1996a) we estimate that, on average, our slit covers approximately one-third

6 454 H. A. Fraquelli, T. Storchi-Bergmann and N. A. Levenson r (parsec) Figure 4. Surface luminosity distribution in Hα (filled symbols), [O III] λ7 (open symbols) and 0-Å continuum (star symbols). Error bars are smaller than the symbols sizes Figure 5. Comparison between Hα and [O III] surface nuclear (NLR) luminosities. The dashed line shows the loci of L area Hα = Larea [O III], for reference. of the area occupied by the emitting gas in the images. Therefore, the total ionized gas mass could be as large as three times the value listed in (3). In order to compare the ionized mass distribution of different galaxies, we have calculated an ionized gas mass per unit area, using the following expression: ( ) L 41 M area H + = Hβ n 1 e M pc 2, (4) A w where A w is the area in square parsecs corresponding to the extraction window (in most cases 2 2 arcsec 2 ). Fig. 6 shows the above mass as a function of distance from the nucleus. In most cases the profiles show a peak on the nucleus, with values between 0.12 and 5.9 M pc 2 and an average of 1.8 ± 1.7 M pc 2, decreasing outwards. In a few cases, the ENLR values are similar to those at the nucleus. We have considered the effect of a larger density for the NLR than that derived from the [S II] ratio in the calculated gas masses. In the extreme case that all the gas has a density of n e = 10 4 cm 3, the NLR masses would decrease typically by one order of magnitude,

7 Table 2. Fitting parameters. L 0 corresponds to the surface luminosities 100 pc from the nucleus. a Extended gas in Seyfert 2 galaxies 455 Galaxy log L 0 δ [O III] log L 0 δ Hα log L 0 δ Cont 0 Å log n 0 [O III] Hα Cont-0 Å [SII] δ ne Table 3. ESO 417-G Fairall CGCG IC AS MCG Mrk Mrk NGC NGC NGC NGC NGC NGC NGC NGC NGC Mrk a In units of erg s 1 pc 2. Ionized gas mass. Id Galaxy Total mass NLR mass (10 3 M ) (10 3 M ) 1 ESO 417-G Fairall CGCG IC AS MCG Mrk Mrk NGC NGC NGC NGC NGC NGC NGC NGC NGC Mrk and become comparable to the values of the windows corresponding to the extranuclear regions. 4 THE IONIZING LUMINOSITY The rate of ionizing photons, Q, intercepted by the gas in each window is related to its Hβ luminosity through the expression (Osterbrock 1989): Q = L Hβα B αhβ eff hν, (5) Hβ where α B is the case B recombination coefficient and α eff Hβ is the effective Hβ recombination coefficient. Table 4 shows the nuclear value, Q nuc (which we consider as corresponding to the unresolved NLR), and the sum of the values from all windows, Q sum (NLR+ENLR). Q sum is the ionizing photon rate one obtains from single-aperture studies (e.g. Kinney et al. 1991), which do not take into account either the dilution of the nuclear radiation with distance from the nucleus or the fact that, for each window, the area facing the source is not totally covered by gas. Q sum thus underestimates the rate of ionizing photons emitted by the source, which we will call Q AGN. In order to obtain Q AGN, it is necessary to take into account the two aspects mentioned above. For a central source emitting Q AGN, the photon rate that crosses the unit area at a distance r from the source is Q AGN /4π r 2. The photon rate intercepted by the gas in each window is proportional to the fraction of its area facing the source that contains gas, which we will call the covering factor of the window C(r) (which is different from the usual definition of the covering factor, the ratio between the solid angle of a gas cloud and 4π). The ionizing photon rate per unit area intercepted by the gas in each window is Q(r) = C(r) Q AGN 4πr 2. (6) Q AGN can thus be obtained for each window Q AGN = Q(r) C(r) 4πr 2 = 4πr 2 L C(r) sup Hβ α B αhβ eff hν, (7) Hβ where we have used equation (5) for Q(r), replacing L Hβ by L sup Hβ = L Hβ /A section, where A section is the area facing the source. This expression considers both the geometric dilution of the nuclear power and the covering factor of the gas facing the source. In order to calculate L sup Hβ, we have adopted two different geometries for each window: (i) a box geometry, where the depth along the line of sight is equal to the linear extent of the window in the plane of the sky; (ii) a conical geometry such that A section = 2 lr tan(θ) (as used by FSBB), where l is the linear extent at the galaxy corresponding to 2 arcsec (slit width), r is the distance between the centre of the window and the source and θ is half the opening angle of the cone of ionizing radiation. We have used θ = 30 as

8 456 H. A. Fraquelli, T. Storchi-Bergmann and N. A. Levenson r (parsec) Figure 6. Ionized gas mass per unit area as a function of the distance from the nucleus. Open symbols show the value for the NLR if N e = 10 4 cm 3 instead of that obtained from the [S II] ratio. representative of the opening angle observed in ionization cones of Seyfert 2 galaxies (Mulchaey, Wilson & Tsvetanov 1996b). In the case of the nuclear extraction (corresponding to the NLR in many cases) we have adopted an effective distance from the ionizing source of 0.5 arcsec, as the extraction window corresponds to 1 arcsec to each side of the nucleus. In the conical geometry we have used A section = πr 2 tan 2 (θ) for the NLR, and L sup Hβ was divided by 2 assuming that we are seeing both sides of the ionization cone. We have first calculated lower limits for Q AGN using equation (7), for each window with C(r) = 1 (which we will call Q AGN ). These values are shown in Fig. 7 for both the box geometry (open circles) and the conical geometry (filled circles). For most galaxies these minimum values derived for all windows are remarkably similar along the ENLR. These similar values suggest that each location absorbs the same number of ionizing photons per unit area. If the gas clouds are ionization-bounded, the assumption of C(r) = 1 within each window is not correct, because it means that the gas should absorb all the ionizing photons and none would reach the subsequent window. However, this cannot be correct because the ionized gas extends to large distances from the nucleus, being present in many subsequent windows implying that the covering factor must be smaller than unity. Indeed, in FSBB it was found that C(r) 0.1 for the ENLR. Thus, in order to calculate the correct value for Q AGN we need to know C(r). 4.1 Covering factor The covering factor C(r) of each window is the fraction of the area facing the ionizing source covered by the gas, and can be calculated as C(r) = A gas(r) A section (r), (8) where A gas is the area effectively occupied by the gas and A section is the area of the geometrical section of the window intercepting the ionizing beam. A section was calculated using the conical geometry (as described in the previous section), and A gas as A gas = M H +η, (9) N H + where M H + is the ionized gas mass in each window (from equation 3) in solar mass units, η is the number of H + ions in one solar mass and N H + is the gas column density.

9 Table 4. Ionizing photons rates Q, covering factor for the NLR, H + column density and spectral indices. Extended gas in Seyfert 2 galaxies 457 Galaxy log Q nuc log Q sum log Q ENLR log Q AGN log Q AGN C NLR log N H + α He II ± σ α α = 1.5 α = 1.5 α He II α He II (cm 2 ) ESO 417-G ± 0.46 Fairall CGCG a a 1.50 ± 0.03 IC ± 0.16 AS ± 0.00 MCG ± 0.27 Mrk ± 0.07 Mrk ± 0. NGC NGC ± 0.02 NGC ± 0.01 NGC ± 0.21 NGC ± 0.17 NGC NGC ± 0.10 NGC ± 0.13 NGC ± 0.30 Mrk ± 0.15 a Maximum log Q AGN obtained along the ENLR assuming C(r) = 1. The value of N H + was obtained using the photoionization code MAPPINGSIc (Binette, Wilson & Storchi-Bergmann 1996), for the gas density obtained in Section 3.2 and assuming a spectral energy distribution L ν ν α, with α = 1.5, for photons with hν 13.6 ev and solar metallicity. For a cloud at a distance r from a source that radiates Q AGN ionizing photons per unit time, the code gives the column N H + for which the ionization fraction H + /H reaches values smaller than 1 per cent of the maximum. The normalization value of the central source luminosity was initially adopted to give the maximum Q AGN along the ENLR under the hypothesis that C(r) = 1. This rate of ionizing photons was then diluted by the distance to each location along the ENLR to obtain N H + in the hypothesis that the clouds are ionization-bounded. For the models to be consistent, the sum of covering factors CENLR (r) along the ENLR cannot exceed unity (for each side of the nucleus). This constraint also ensures that the central source generates the necessary number of photons to ionize the entire ENLR. Only for Mrk 607, MCG , AS , Fairall 316, ESO 417-G6 and Mrk 348 did we obtain C ENLR (r) 1. In the remaining cases, we originally found it to be larger than unity. We have thus increased the luminosity of the central source until CENLR (r) 1. The resulting number of ionizing photons per unit time Q ENLR obtained as the sum of the contributions from all windows is also shown in Table 4. We have next included the contribution of the nuclear extraction (NLR) in the calculations with the constraint that C ENLR + C NLR 1. Fig. 8 shows the C NLR value and the C ENLR distributions along the ENLR. The values for the NLR range from 0.2 to 0.8, while for the ENLR the average value is C(r) = 0.1 (as in FSBB). 4.2 Nuclear ionizing photon rate Q AGN Adding the contributions from both the NLR and the ENLR we have derived the total number of ionizing photons Q AGN, shown in Table 4 and as dashed line in Fig. 7. This number ranges from to photon s 1 (with an average value of Q = ±1.7 photon s 1 ). We also list in Table 4 the total ionized gas column, calculated as N H + = C(r)NH + C(r). (10) The actual source could be even more luminous if some photons escape or are not detected. We thus regard all values of Q in Table 4 as minimum values. A comparison between Q ENLR and Q AGN shows that, on average, two-thirds of the ionizing photons are absorbed in the ENLR and the remaining one-third in the NLR. The Q AGN value quoted in Table 4 can be compared with Q sum. The latter, which has been frequently used in previous works to estimate the nuclear source luminosity, underestimates Q AGN by approximately one order of magnitude. This is illustrated in Fig. 9, which shows the relation between the total Hα luminosity (NLR+ENLR) and both Q sum and Q AGN. A linear regression to the relation between Q AGN and the total Hα luminosity gives log Q AGN = log L tot Hα (11) for L tot Hα in erg s 1. This relation can be used to estimate the number of ionizing photons per unit time of a nuclear source once the Hα luminosity is known. 4.3 Effects of a different SED on Q AGN Previous studies, for example Cid Fernandes et al. (1998) and Storchi-Bergmann et al. (2000), identified circumnuclear starbursts in four of our sample galaxies: NGC 5135, 7130, 7582 and Mrk In the cases of NGC 5135 and 7130 the bolometric luminosity of the starburst seems to be comparable to that of the AGN (González-Delgado, Heckman & Leitherer 2001). In order to investigate the implication of the above result we have calculated the bolometric luminosities of a starburst with an SED given by Schmitt et al. (1997) and that of an AGN with an SED given by Elvis et al. (1994) for radio-quiet quasars. For equal values of bolometric luminosities we obtained that 35 per cent of the number of ionizing photons per second is contributed by the starburst. Thus, the values of Q AGN could be down to 65 per cent of the values listed in Table 4 for NGC 5135 and The same should apply to NGC 7582 and Mrk 1210.

10 458 H. A. Fraquelli, T. Storchi-Bergmann and N. A. Levenson r (parsec) Figure 7. Minimum rate of ionizing photons Q AGN radiated by the AGN calculated from the Hβ luminosities of each window for C(r) = 1 and both the conical geometry (filled symbols) and box geometry (open symbols). The long dashed line represents the value of the total rate of ionizing photons Q AGN calculated in Section 4.1. We have also investigated the effects of a higher gas density for the NLR than that obtained from the [S II] ratio. For n e = 10 4 cm 3, the resulting C NLR are 10 per cent smaller and the effect in log Q AGN is to decrease its value by at most 0.2 dex. In addition, we have tested other values of α besides 1.5 and verified that C does not vary much: the value of C for α = 1.5 is 40 per cent larger than that for α = 1.0 and 20 per cent smaller than that for α = He + ionizing photons The luminosity in the He II λ4686 emission line can be used to calculate the rate at which ionizing photons with hν 54.4 ev reach each window. Similarly to equation (5), for He II λ4686 we have (Osterbrock 1989) Q(He + ) = L He +αhe+ B, (12) α eff He hν + He + where α He+ B is the He II recombination coefficient in case B and α eff He + is the effective He II λ 4686 recombination coefficient. For the locations in which we measure both He II and Hβ emission we can derive the slope α He II of the ionizing continuum between 13.6 and 54.4 ev, under the assumption that L ν ν α He II. The slope is given by α He II = log [ Q(H + )/Q(He + ) ]. (13) log 4 The values derived for α He II using the expression above are listed in the final column of Table 4. The average for the whole sample is α He II = 1.3 ± 0.3. However, instead of being evenly spread around the average, the α He II values seem to cluster around two values: α He II = 1.6 ± 0.1 (eight cases) with values varying from 1.46 to 1.76 and α He II = 1.0 ± 0.1 (six cases) with values varying from 0.82 to We note that four of the eight galaxies with softer ionizing spectra are those with circumnuclear starbursts (see the previous section), in which part of the ionization is caused by young stars. Using the starburst models of Leitherer & Heckman (1995), we verified that the predicted α He II using equation (13) for a pure starburst is 1.66, consistent with an important contribution of the starburst in the above four cases.

11 Extended gas in Seyfert 2 galaxies Figure 8. r (parsec) Figure 9. Q sum (dashed line) and Q AGN (filled circles) versus the total Hα luminosity. The solid line shows a linear regression to the latter relation. Covering factor distributions. We have repeated the calculations of Q AGN using the derived value of α He II instead of the adopted α = 1.5 in the previous calculations. This value is also shown in Table 4, together with the corresponding C NLR. The new values of Q AGN and C NLR do not differ much from previous values, confirming that they are not strongly dependent on the value of α, but should be considered more robust because the observations constrain them. Fig. 10 shows the relation between α He II and the highest value of [O III]/Hβ obtained along the NLR+ENLR. This figure shows a trend for the harder continua to be associated with higher values of the [O III]/Hβ ratio. 5 COMPARISON OF THE PREDICTED IONIZING LUMINOSITY WITH OBSERVED HARD -RAY LUMINOSITIES In this section we use the derived spectral shape and ionizing luminosity to predict the intrinsic -ray emission of the galaxy nuclei. In Seyfert 2s, much of this high-energy flux will be absorbed, either by material very close to the nucleus the torus of the unified model scenario or other gas in these galaxies, and will therefore not emerge in -rays. With sufficiently low column densities

12 460 H. A. Fraquelli, T. Storchi-Bergmann and N. A. Levenson Figure 10. The spectral index α He II versus the [O III]/Hβ ratio. (N H < cm 2 ), however, we will detect some of this intrinsic emission directly, particularly at higher energies. In order to predict the intrinsic -ray luminosity in the 2 10 kev band, L pred, we apply the spectral slope α He II appropriate from 13.6 to 54.4 ev that we determined from the He II/Hβ ratio normalized at 13.6 ev by the ionizing luminosity derived from Q AGN, and then extrapolate this SED to -ray energies. Such an extrapolation has been previously successfully applied to individual galaxies using detailed photoionization modelling (e.g. Alexander et al. 1999). The values of L pred are listed in Table 5. We compare the predicted intrinsic luminosities with ASCA -ray observations of our sample. We use the reduced data of Levenson, Weaver & Heckman (2001) for NGC 5135, 7130 and 7582, the reduced spectra from the TARTARUS data base for Mrk 1210, NGC 1386, 5643 and Mrk 348, and the spectra extracted in standard ASCA processing for NGC 1358 and The most important spectral components are the buried intrinsic AGN, which we model as a power law, and the scattered AGN contribution, which we model as a power law of the same spectral index, though absorbed only by the Galactic column density. In each case, we fix the spectral index Table 5. H I column densities N H (all in units of cm 2 ). Galaxy log N Gal H log L obs log L ac log N H log L pred log N pred H (cm 2 ) (erg s 1 ) (erg s 1 ) (cm 2 ) (erg s 1 ) (cm 2 ) ESO 417-G Fairall CGCG IC AS MCG Mrk Mrk NGC NGC > NGC NGC NGC a a > NGC NGC NGC > NGC Mrk a Excluding the Fe Kα line. to the value of α He II measured above. Some cases require Fe Kα fluorescence lines at E 6.4 kev. Additional soft components may be present, owing to a thermal starburst or individual sources in the disc of a galaxy, for example. We neglect these in general, however, because we are primarily concerned with higher energies, although we do adopt the more complex best-fitting models of Levenson et al. (2001) in those cases. We fit these models to the data to determine the observed -ray luminosity, L obs, and the column density to the AGN, N H, which are listed in Table 5. We correct for this measured obscuration to obtain the absorption-corrected -ray luminosity, L ac, to estimate the intrinsic luminosity of the buried AGN. For the galaxies with N H <10 24 cm 2, the correction to the measured absorption recovers the intrinsic -ray emission well because the AGN is directly detected at high energies. In these cases, we find that the spectral extrapolation from the optical and ultraviolet (UV) regime provides a good estimate of the high-energy emission of the AGN. In the Compton-thick galaxies, which have N H > cm 2, the buried AGN is not directly measured within the ASCA bandpass. In these cases, all the observed 2 10 kev luminosity is caused by the scattered component or additional sources within each galaxy and is not directly related to the total output of the central engine. Single power-law spectral models characterize these examples, typically with the measured N H = N G H (the H I column density from our galaxy), which further implies that we detect only the scattered continuum component. Thus, we expect that L ac severely underpredicts the true -ray flux. Indeed, we find L ac Lpred in these cases and suggest that L pred provides an estimate of the intrinsic -ray emission in Compton-thick galaxies. We also use L pred to derive the column density from an observed -ray luminosity, even if an -ray spectrum is not available. In terms of σ E, the photoelectric cross-section of Morrison & McCammon (1983), L obs = Lpred e Npred H σe. (14) Integrating over the expected power-law SED we obtain the N pred H values shown in Table 5, corrected for the Galactic column density. We compare N pred H with the values obtained through -ray

13 Figure 11. Comparison between N pred H and N H. See Table 1 for galaxy identifications. spectroscopy in Fig. 11. While this method yields reasonable values of N H in the Compton-thin cases, it does not accurately measure N H > cm 2, although it does correctly identify them as being Compton-thick. Fundamentally, equation (14) is inapplicable to the latter because the origin of the detected -rays, even at energies up to 10 kev, is not the obscured AGN. With these results, we are confident that the -ray luminosities predicted from the optical and UV ionizing continuum are reliable estimates of the intrinsic -ray luminosity. If -ray fluxes are measured, these can be compared to determine the absorbing column density reasonably well for N H < cm 2, or correctly identify the Compton-thick cases. Finally, we compare the neutral column densities along the line of sight to the AGN with the ionized column densities along the ENLR obtained in Section 4.1. The latter range from to cm 2, values that are typical of the ionized column densities measured in Seyfert 1 galaxies (Reynolds 1997; George et al. 1998), but two orders of magnitude smaller than the neutral column densities in our sample of Seyfert 2s. Even accounting for the neutral gas contribution in our adopted model of ionization-bounded clouds, the total column density of material along the ENLR is still <10 22 cm 2. Thus, when the central engines are viewed along the ENLR line of sight, nearly all the hard -rays emerge unobscured, consistent with what is observed in Seyfert 1 galaxies. Medium-to-high luminosity AGNs present a big blue bump in the spectral range 14.5 log ν(hz) 16.5 (Elvis et al. 1994). It is difficult to conclude whether or not the big blue bump is present in our sample of galaxies. However, our success in predicting the hard -ray luminosities using the extrapolated ionizing UV SED may suggest that the SED of our sample are different from the average one of radio-quiet quasars from Elvis et al. (1994, their fig. 10). On the other hand, we have noticed that if we use the average α He II = 1.3 in the radio-quiet high-luminosity AGN SED from Elvis et al. to extrapolate the near-uv SED (at 912 Å) to the hard -rays domain we still approximately recover its 4-keV luminosity (within 30 per cent). 6 COMPARISON BETWEEN THE PREDICTED INFRARED LUMINOSITY AND OBSERVED AS LUMINOSITY Another spectral range for which observations of the central luminosity are available although reprocessed is the infrared () Extended gas in Seyfert 2 galaxies 461 AS domain. Under the assumption that most of the optical and ultraviolet radiation is absorbed by a dusty torus surrounding the nuclear source, the dust grains near the nucleus will reradiate this energy in the. Following the approach of Storchi-Bergmann, Mulchaey & Wilson (1992b), we now compare the observed infrared luminosities with the predicted ones, as follows. Assuming that the ionizing source is an isotropic radiator and that a dusty torus absorbs all photons incident on it in the wavelength range 100 Å 1 µm, the predicted luminosity L pred for the torus is given by L pred = LPL = (1 C cone)q AGN h ανα 0 (1 α) ( ) ν 1 α 2 ν 1 α 1, (15) where C cone = 1 cos(θ) is the covering factor of the bicone of escaping radiation with θ = 30 (see Section 4), h is the Planck constant, ν 0 = Hz (λ = 912 Å), ν 1 = Hz (λ = 1 µm), ν 2 = Hz (λ = 100 Å) and α He II is the slope of the SED derived in Section 4.4 (listed in Table 4). The above approach assumes that the non-ionizing SED is an extrapolation of the ionizing one. However, this may not be the case, as the SED is not readily observable in Seyfert 2 galaxies. We have thus repeated the above calculation for a non-ionizing part of the SED as given by the average one of Elvis et al. (1994) for radio-quiet quasars, which we have approximated by three segments (hereafter Elvis SED): the first from ν 2 to ν 3 = Hz; the second from ν 3 to ν 4 = Hz and the third from ν 4 to ν 1. In this case, L pred = LElvis = (1 C cone )Q AGN h(s1 + s2 + s3), (16) where αν α ( 0 s1 = ν 1 α He II ) 2 ν 1 α He II 3 (1 α He II ) (17) ( ν3 ) αhe II s2 = ν3 ln(ν 3 /ν 4 ) ν 0 (18) s3 = να ( 4 ν 1 α ) 4 ν 1 α 1 1 α (19) and α = 0.7. The results for L PL and LElvis are listed in Table 6. The values for L PL are larger than those for LElvis (1.1 <L PL /LElvis < 2.7), as the power-law adopted in the first case predicts larger non-ionizing fluxes than the Elvis SED. AS fluxes are available for 14 galaxies of our sample, which we obtained from the NASA-IPAC Extragalactic Data base (NED). We have calculated the integrated AS fluxes for each AS band as in Rowan-Robinson & Crawford (1989). Using the 12- and 25- µm fluxes we have calculated the warm AS luminosity, L warm, and also using the 60- and 100-µm fluxes, the total AS luminosity, L tot, which are listed in Table 6. We show in Fig. 12 a comparison of L pred with L tot, where open symbols correspond to the power-law SED while filled symbols correspond to Elvis SED. This figure shows that the predicted luminosities are consistent with the observed ones, supporting the adopted simple reradiation model. However, following the discussion of Storchi-Bergmann et al. (1992), we expect that the observed luminosity should be equal to or larger than the predicted luminosity for the torus (because of the large AS beam, extranuclear sources, such as star-forming regions, may contribute to the AS fluxes). A closer look at Fig. 12 shows that L PL in fact overpredicts the infrared luminosity for the higher-luminosity objects, and in light of the above discussion, the Elvis SED gives a better prediction for the infrared luminosity.

14 462 H. A. Fraquelli, T. Storchi-Bergmann and N. A. Levenson Table 6. properties. Galaxy log L warm log L tot log L PL log L Elvis (erg s 1 ) (erg s 1 ) (erg s 1 ) (erg s 1 ) -0.2 ESO 417-G Fairall CGCG IC AS MCG Mrk Mrk NGC NGC NGC NGC NGC NGC NGC NGC NGC Mrk Figure 12. L tot filled symbols to L pred versus Lpred. Open symbols correspond to Lpred = LElvis. = LPL and L warm also increases with L pred. If the luminosity is dominated by reprocessed radiation from the torus, this is exactly what we expect. In Fig. 13 we plot the dependence of the ratio L warm /L tot on (where open symbols correspond to the power-law SED while L pred filled symbols correspond to the Elvis SED). This shows that, for most galaxies, L warm /L tot increases with Lpred, indicating that Lwarm is dominated by reprocessed nuclear radiation. The three galaxies that do not follow the above behaviour are NGC 5135, 7130 and 7582, which have a small L warm /L tot for their Lpred. These galaxies have composite Seyfert 2 + starburst nuclei, as discussed in previous sections, thus their behaviour can be understood as arising from the large contribution of the circumnuclear starburst, which increases the 60- and 100-µm luminosities and decreases L warm /L tot.ifwe assume that the AGN in these galaxies follows the same relation between L warm /L tot and Lpred as the other galaxies without a circumnuclear starburst, then log(l warm /L tot ) 0.2 for the AGN. We can then derive the relative contribution of the AGN and star Figure 13. L warm /L tot versus Lpred (see the Table 1 for galaxy identifications). Symbols as in Fig. 12. burst in the AS domain, which is L AGN cases above. /LSB 0.5 for the three 7 SUMMARY AND CONCLUDING REMARKS We have used optical long-slit spectroscopy to investigate the properties of the NLR and ENLR of a sample of 18 nearby Seyfert 2 galaxies and to obtain the luminosities of the central sources. The properties of the ENLR were measured within extraction windows corresponding to linear extents at the galaxies in the range pc. The NLR is usually included in the nuclear extraction. Extended emission was observed up to typically 2 kpc from the nucleus, and in a few cases up to 4 kpc. The reddening distribution shows, for approximately half the galaxies for which it could be obtained, smaller values for the NLR than for neighbouring locations of the ENLR. This result could be caused by destruction of the dust by the AGN radiation or optical depth effects, such that only the less obscured regions are observed (Veilleux et al. 1995). The average density of the NLR is 400 cm 3, and decreases along the ENLR where it reaches the low-density limit. The [O III] line emission distribution is, on average, more centrally peaked than those of [O II] and Hα. This is caused by a higher excitation closer to the nucleus and decreasing outwards and/or to the contribution of other lower ionization sources (e.g. H II regions) in the outer regions to the [O II] and Hα line emission. The total masses of ionized gas are in the range M. We have used the Balmer emission-line luminosities of both the NLR and ENLR to derive the rate of ionizing photons radiated by the central source. We have taken into account the geometrical dilution of the nuclear source radiation and assumed that the gas in each extraction window is ionization-bounded. The values obtained for the total number of ionizing photons vary from to photon s 1, and are, on average, one order of magnitude larger than those that would be obtained merely by integrating the total observed Balmer emission-line luminosities as performed in previous works. The total rate of ionizing photons Q AGN scales with the total (NLR+ENLR) Hα luminosity, which can be used as a calibrator for obtaining Q AGN.Wefind that the average value for the covering factor of the gas in each window along the ENLR is 0.1. The spectral slope between 13.6 and 54.4 ev measured using the He II/Hβ ratio was used to extrapolate the SED (adopting a power law) from the ionizing UV to hard -ray domain and to calculate the